Testing galaxy feedback models with the first resolved profiles of the circumgalactic medium. (arXiv:2203.01356v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Chadayammuri_U/0/1/0/all/0/1">Urmila Chadayammuri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bogdan_A/0/1/0/all/0/1">Akos Bogdan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oppenheimer_B/0/1/0/all/0/1">Benjamin Oppenheimer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">Ralph Kraft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forman_W/0/1/0/all/0/1">William Forman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_C/0/1/0/all/0/1">Christine Jones</a>
The hot ($>10^6$ K) phase of the circumgalactic medium (CGM) contains a large
fraction of baryons in galaxies. It also retains signatures of the processes
that shaped the galaxies, such as feedback from active galactic nuclei (AGNs)
and supernovae, and offers a uniquely powerful way to constrain theoretical
models of feedback. It is, however, notoriously difficult to detect. By
stacking 2643 optically selected galaxies in the eROSITA Final Equatorial Depth
Survey (eFEDS), we present spatially resolved properties of the extended CGM in
both star-forming and quiescent galaxies spanning an order of magnitude in
stellar mass. We mask out resolved point sources and galaxy groups/clusters and
model the contribution from X-ray binaries and the hot ISM, producing accurate
radial profiles. We compare the profiles to mock X-ray observations of galaxy
stacks in the IllustrisTNG100 (TNG) and EAGLE cosmological simulations. We
detect extended emission from both the high-mass
($10.7<log(M_*/M_odot)<11.2$) and low-mass ($10.2<log(M_*/M_odot)<10.7$)
galaxy stacks. Galaxies have somewhat more luminous CGM between $10-100$~kpc if
they are more massive or star-forming. However, the luminosity increases slower
with stellar mass than predicted in simulations. Simulated quenched galaxies
are far dimmer than observed, suggesting that they rely too heavily on CGM
ejection for quenching. Star-forming galaxies are observed to have flatter and
more extended profiles than in simulations, suggesting under-efficient stellar
feedback models. Our results highlight the need to modify future prescriptions
of galaxy feedback models.
The hot ($>10^6$ K) phase of the circumgalactic medium (CGM) contains a large
fraction of baryons in galaxies. It also retains signatures of the processes
that shaped the galaxies, such as feedback from active galactic nuclei (AGNs)
and supernovae, and offers a uniquely powerful way to constrain theoretical
models of feedback. It is, however, notoriously difficult to detect. By
stacking 2643 optically selected galaxies in the eROSITA Final Equatorial Depth
Survey (eFEDS), we present spatially resolved properties of the extended CGM in
both star-forming and quiescent galaxies spanning an order of magnitude in
stellar mass. We mask out resolved point sources and galaxy groups/clusters and
model the contribution from X-ray binaries and the hot ISM, producing accurate
radial profiles. We compare the profiles to mock X-ray observations of galaxy
stacks in the IllustrisTNG100 (TNG) and EAGLE cosmological simulations. We
detect extended emission from both the high-mass
($10.7<log(M_*/M_odot)<11.2$) and low-mass ($10.2<log(M_*/M_odot)<10.7$)
galaxy stacks. Galaxies have somewhat more luminous CGM between $10-100$~kpc if
they are more massive or star-forming. However, the luminosity increases slower
with stellar mass than predicted in simulations. Simulated quenched galaxies
are far dimmer than observed, suggesting that they rely too heavily on CGM
ejection for quenching. Star-forming galaxies are observed to have flatter and
more extended profiles than in simulations, suggesting under-efficient stellar
feedback models. Our results highlight the need to modify future prescriptions
of galaxy feedback models.
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